Early evolution of newly born magnetars with a strong toroidal field

Dall’Osso, S.; Shore, Steven N.; Stella, L.

doi:10.1111/j.1365-2966.2008.14054.x

Cited by 156 publications

(227 citation statements)

References 81 publications

(185 reference statements)

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“…Our observational constraints would also be weakened if a large fraction of the magnetar rotational energy is emitted as gravitational waves instead of through electromagnetic spindown (e.g., Doneva et al 2015;Gao et al 2016;Lasky & Glampedakis 2016). This could occur either due to a misalignment between the rotation axis and the magnetic dipole axis (e.g., Dall'Osso et al 2009) or via the growth of the f-mode instability (e.g., Doneva et al 2015). However, Figure 4.…”

Section: Discussionmentioning

confidence: 90%

Radio Constraints on Long-Lived Magnetar Remnants in Short Gamma-Ray Bursts

Fong

Metzger

Berger

et al. 2016

ApJ

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The merger of a neutron star (NS) binary may result in the formation of a rapidly spinning magnetar. The magnetar can potentially survive for seconds or longer as a supramassive NS before collapsing to a black hole if, indeed, it collapses at all. During this process, a fraction of the magnetar's rotational energy of ∼10 53 erg is transferred via magnetic spin-down to the surrounding ejecta. The resulting interaction between the ejecta and the surrounding circumburst medium powers a year-long or greater synchrotron radio transient. We present a search for radio emission with the Very Large Array following nine short-duration gamma-ray bursts (GRBs) at rest-frame times of ≈1.3-7.6 yr after the bursts, focusing on those events that exhibit early-time excess X-ray emission that may signify the presence of magnetars. We place upper limits of 18-32 μJy on the 6.0 GHz radio emission, corresponding to spectral luminosities of (0.05-8.3)×10 39 erg s −1 . Comparing these limits to the predicted radio emission from a long-lived remnant and incorporating measurements of the circumburst densities from broadband modeling of short GRB afterglows, we rule out a stable magnetar with an energy of 10 53 erg for half of the events in our sample. A supramassive remnant that injects a lower rotational energy of 10 52 erg is ruled out for a single event, GRB 050724A. This study represents the deepest and most extensive search for long-term radio emission following short GRBs to date, and thus the most stringent limits placed on the physical properties of magnetars associated with short GRBs from radio observations.

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Section: Discussionmentioning

confidence: 90%

Radio Constraints on Long-Lived Magnetar Remnants in Short Gamma-Ray Bursts

Fong

Metzger

Berger

et al. 2016

ApJ

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“…Additional mechanisms have been proposed, which might be initially more efficient in extracting the NS spin energy and angular momentum, as long as it spins at 1 ms (cf. Bucciantini et al 2006Bucciantini et al , 2008Dall'Osso et al 2009;Metzger 2010). We finally note that in at least one case (GRB060729), the X-ray luminosity at late times is somewhat lower than the model prediction.…”

Section: Comparison With Observations and Resultsmentioning

confidence: 99%

“…Different possibilities for this to occur have been investigated in the literature (Palomba 2001;Cutler 2002;Stella et al 2005;Dall'Osso & Stella 2007;Dall'Osso et al 2009;Corsi & Meszaros 2009) showing that in astrophysically plausible conditions, GW emission might efficiently extract spin energy from the NS, in competition with magnetic dipole losses. The study presented here builds on the ansatz that millisecond spinning magnetars are formed in the events that give rise to long GRBs.…”

Section: Introductionmentioning

confidence: 99%

Gamma-ray bursts afterglows with energy injection from a spinning down neutron star

Dall’Osso

Stratta²,

Guetta

et al. 2011

A&A

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175

157

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Aims. We investigate a model for the shallow decay phases of gamma-ray burst (GRB) afterglows discovered by Swift/XRT in the first hours following a GRB event. In the context of the fireball scenario, we consider the possibility that long-lived energy injection from a millisecond spinning, ultramagnetic neutron star (magnetar) powers afterglow emission during this phase. Methods. We consider the energy evolution in a relativistic shock that is subject to both radiative losses and energy injection from a spinning down magnetar in spherical symmetry. We model the energy injection term through magnetic dipole losses and discuss an approximate treatment for the dynamical evolution of the blastwave. We obtain an analytic solution for the energy evolution in the shock and associated lightcurves. To fully illustrate the potential of our solution we calculate lightcurves for a few selected X-ray afterglows observed by Swift and fit them using our theoretical lightcurves. Results. Our solution naturally describes in a single picture the properties of the shallow decay phase and the transition to the socalled normal decay phase. In particular, we obtain remarkably good fits to X-ray afterglows for plausible parameters of the magnetar. Even though approximate, our treatment provides a step forward with respect to previously adopted approximations and provides additional support of the idea that a millisecond spinning (1-3 ms), ultramagnetic (B ∼ 10 14 −10 15 G) neutron star loosing spin energy through magnetic dipole radiation can explain the luminosity, durations and shapes of X-ray GRB afterglows.

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“…Furthermore, seismic, thermal, and quantum noises reduce the sensitivity of GW detectors at low frequencies, ν 10 Hz (Abbott et al 2010;Hild et al 2011). Hence, traditionally Galactic magnetars are not considered to be prime targets, although newborn magnetars are more promising (Thompson et al 2004;Stella et al 2005;Dall'Osso et al 2009). …”

Section: Gravitational Radiationmentioning

confidence: 99%

Gravitational radiation from neutron stars deformed by crustal Hall drift

Suvorov

Mastrano

Geppert

2016

Mon. Not. R. Astron. Soc.

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A precondition for the radio emission of pulsars is the existence of strong, small-scale magnetic field structures ('magnetic spots') in the polar cap region. Their creation can proceed via crustal Hall drift out of two qualitatively and quantitatively different initial magnetic field configurations: a field confined completely to the crust and another which penetrates the whole star. The aim of this study is to explore whether these magnetic structures in the crust can deform the star sufficiently to make it an observable source of gravitational waves. We model the evolution of these field configurations, which can develop, within ∼ 10 4 -10 5 yr, magnetic spots with local surface field strengths ∼ 10 14 G maintained over 10 6 yr. Deformations caused by the magnetic forces are calculated. We show that, under favourable initial conditions, a star undergoing crustal Hall drift can have ellipticity ∼ 10 −6 , even with sub-magnetar polar field strengths, after ∼ 10 5 yr. A pulsar rotating at ∼ 10 2 Hz with such is a promising gravitational-wave source candidate. Since such large deformations can be caused only by a particular magnetic field configuration that penetrates the whole star and whose maximum magnetic energy is concentrated in the outer core region, gravitational wave emission observed from radio pulsars can thus inform us about the internal field structures of young neutron stars.

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Early evolution of newly born magnetars with a strong toroidal field

Cited by 156 publications

References 81 publications

Radio Constraints on Long-Lived Magnetar Remnants in Short Gamma-Ray Bursts

Radio Constraints on Long-Lived Magnetar Remnants in Short Gamma-Ray Bursts

Gamma-ray bursts afterglows with energy injection from a spinning down neutron star

Gravitational radiation from neutron stars deformed by crustal Hall drift

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